We take the line-of-sight velocity dispersion profiles for the kinematic distance fitting from [1]}, [2]} and [3]}. [1]}
calculated line-of-sight velocity dispersion profiles by combining literature velocities with line-of-sight velocities derived from archival spectra from the ESO and Keck data archives.
[2]} and [3]} added line-of-sight velocities from Gaia DR2 and the Anglo-Australian Observatory (AAO) data archive to these profiles. In
addition we use the line-of-sight
velocity dispersion profiles published by [7]} based on MUSE data. We take the proper motion dispersion
profiles either from VB21 based on Gaia EDR3 data, or from published profiles based on multi-epoch HST measurements. Table REF  lists
the HST proper motion velocity dispersion profiles that we use in this paper together with the distances that we derive from these profiles. Unfortunately we could not use the recently
published proper motion dispersion profiles for nine inner Milky Way globular clusters by [8]} since no accurate line-of-sight velocity dispersion profiles are available for these clusters.
<TABLE>